标题： 高银道面脉冲星\snr 的多波长研究 显示英文标题

标题： Multi-wavelength study of the high Galactic latitude supernova remnant candidate \snr\ associated with the Calvera pulsar

摘要： 候选超新星遗迹（SNR）G118.4+37.0（Calvera的SNR），在高银河纬度处被发现为一个微弱的射电环，并与扩展的费米/LAT伽马射线辐射相重合，可能与X射线脉冲星1RXS J141256.0+792204（Calvera）有关。 之前的XMM-Newton数据提示环内存在软的弥散X射线辐射，但曝光不足，无法详细表征。 我们获得了新的XMM-Newton观测数据，并生成了计数率图像、等效宽度和中位光子能量图，以确定最佳的光谱分析区域。 我们补充了对费米/LAT伽马射线数据的重新分析以及新的国家天文台望远镜观测，旨在搜索Halpha发射。 X射线弥散辐射可以用一个温度kT\sim 0.15 keV的激波加热等离子体模型很好地描述，其N和O丰度略低于太阳值，电子密度ne=0.1-0.7 cm-3。 根据我们的估计，Calvera的SNR年龄为10-20 kya，距离为4-5 kpc。 一个明显的“团块”区域显示出同样可以用热模型（kT\sim 1.7 keV）或非热模型（Gamma\sim 2.7）很好描述的发射。 最亮的X射线区域靠近伽马射线峰值和一个孤立的Alpha丝状结构。 G118.4+37.0是一个中年遗迹，在稀薄介质中膨胀，并遇到了更密集的区域，可能是大质量前身星风活动的残余。 估计的SNR距离在不确定范围内与Calvera的距离估计一致，确认了这个特殊的脉冲星是在银河盘上方的大质量恒星爆炸中诞生的。 我们测量的环境密度，加上伽马射线辐射的斑驳形态和Halpha丝状结构的检测表明，强子起源与伽马射线通量相容，尽管不能排除混合的轻子-强子起源。 显示英文摘要

摘要： The candidate supernova remnant (SNR) G118.4+37.0 (Calvera's SNR), discovered as a faint radio ring at high Galactic latitude and coincident with extended Fermi/LAT gamma-ray emission, is likely associated to the X-ray pulsar 1RXS J141256.0+792204 (Calvera). Previous XMM-Newton data hinted at soft diffuse X-ray emission inside the ring but lacked sufficient exposure for detailed characterisation. We obtained new XMM-Newton observations, and produced count-rate images, equivalent width and median photon energy maps to identify optimal regions for spectral analysis. We complemented these observations with a reanalysis of Fermi/LAT gamma-ray data and new Telescopio Nazionale Galileo observations aimed to search for Halpha emission. The X-ray diffuse emission is well described by a model of shock-heated plasma with temperature kT \sim 0.15 keV, mildly under-solar N and o abundances and densities ne=0.1-0.7 cm-3. According to our estimates, Calvera's SNR is 10-20 kya old and lies at a distance of 4-5 kpc. A distinti "Clump" region shows hared emission equally well described by a thermal (kT\sim 1.7 keV) or a non thermal model (Gamma \sim 2.7). The brightest X-ray area is close to the gamma-ray peak and to an isolated Alpha filament. G118.4+37.0 is a middle-aged remnant which expands in a tenuous medium and encountered a denser phase, likely the relic of the wind activity of the massive progenitor star. The estimated SNR distance is consistent within the uncertainties with that estimated for Calvera, confirming that this peculiar pulsar was born in the explosion of a massive star high above the Galactic disk. Our measured ambient density, together with the patchy morphology of the gamma-ray emission and the detection of Halpha filaments indicates that a hadronic origin is compatible with the gamma-ray flux, though a mixed leptonic-hadronic cannot be excluded